FIRE PROTECTION SYSTEMS CATALOG SYSTEMS PROTECTION FIRE Effective March 2018 March Effective

Total Page:16

File Type:pdf, Size:1020Kb

FIRE PROTECTION SYSTEMS CATALOG SYSTEMS PROTECTION FIRE Effective March 2018 March Effective FIRE PROTECTION VICTAULIC SYSTEMS CATALOG Effective March 2018 ® FIRE PROTECTION SYSTEMS CATALOG Effective March 2018 U.S./World Headquarters EMEAI Asia Pacific 4901 Kesslersville Road Prijkelstraat 36 Unit 808, Building B Easton, PA 18040 USA 9810 Nazareth, Belgium Hongwell International Plaza No.1602 West Zhongshan Road victauliclocations.com Shanghai, China 200235 G-105 3567 REV I 03/2018 Victaulic and all other Victaulic marks are the trademarks or registered trademarks of Victaulic Company, and/or its affiliated entities, in the U.S. and/or other countries. All other trademarks listed herein are the property of their respective holders, in the U.S. and/or other countries. The terms “Patented” or “Patent Pending” refer to design or utility patents or patent applications for articles and/or methods of use in the United States and/or other countries. © 2018 VICTAULIC COMPANY. ALL RIGHTS RESERVED. Intro Regulatory Compliance Victaulic piping system products are VdS – Verband der HVAC Pressure Equipment Safety tested and certified for a wide range Schadenverhütung GmbH (Germany) CSTB – Centre Scientifique et (2014/68/EU) PED – Pressure of applications. Victaulic engages VicFlex with many certifying authorities, VKF – Vereinigung Kantonaler Technique du Bâtiment (France) Equipment Directive (Europe) Feuerversicherungen (Switzerland) approval bodies, and standards ITB – Instytut Techniki Budowlanej CSA B51 – "Boiler, Pressure Vessel, ™ organizations globally, and maintains Zagrebinspekt (Croatia) (Poland) and Pressure Piping Code" (Canada) product certifications and strict compliance to applicable codes, Sercons Europe BV (Russia) CRN – Canadian Registration Potable Water Numbers per CSA B51 Couplings standards, and directives, relevant to specific industries and markets. ARPA – Agenzia Regionale per Plumbing CU TR 032/2013 – Customs Union la Protezione dell’Ambiente (Italy) Technical Regulation “On Safety IAPMO – International Association of Pressurized Equipment” (EAC) PRODUCT CERTIFICATIONS: Belgaqua – Belgische Federatie of Plumbing & Mechanical voor de Watersector (Belgium) Officials (USA) Chemical Safety / Recycling Fittings Fire Protection DVGW – Deutscher Verein des Gas- NSF – NSF International (USA) und Wasserfaches e.V. (Germany) BVB – Byggvarubedömningen ACTIVFIRE – ActivFire Register Service AB (Sweden) of Fire Protection Equipment Eurofins – ACS : Attestation de (Australia) Conformité Sanitaire (France) (EC/1907/2006) REACH – Registration, Evaluation, FireLock AON – AON New Zealand HZJZ – Hrvatski zavod za javno COMPLIANCE: Authorization, and Restriction zdravstvo (Croatia) CCCF – China Certification Center of Chemicals (Europe) ™ for Fire Protection Products (China) INSP - Institutul Naţional De Codes and Standards Compliance (2011/65/EU) RoHS2 – Restriction IGS Sănătate Publică (Romania) CFPSC – Chinese Fire Protection ANSI – American National of Hazardous Substances Safety Center (Taiwan) KWWA – Korea Water and Standards Institute Directive (Europe) Wastewater Works Association Hole Cut CNBOP – Centrum Naukowo- API – American Petroleum Institute (2012/19/EU) WEEE – Waste Badawcze Ochrony NSF – NSF International (USA) Electrical and Electronic Przeciwpozarowej (Poland) APSAD – Assemblée Plenière Equipment Directive (Europe) ÖVGW – Österreichische Société Assurance Dommage CNPP – Centre National de Vereinigung für das Gas- (France) SundaHus – SundaHus i Linköping (Sweden) Prévention et de Protection und Wasserfach (Austria) Accessories (France) AS/NZS – Standards Australia and Valves and PZH – Państwowy Zakład Standards New Zealand CSFM – California State Fire Higieny (Poland) (AU & NZ) Building Services Marshall (USA) RUVZPP – Regionálny úrad ASME – American Society of (EU/305/2011) CPR – Construction CTPC – Consiliul Technic verejného zdravotníctva so Mechanical Engineers (USA) Products Regulation (Europe) Devices and Permanent Pentru Constructii sídlom v Poprad (Slovakia) NBC – National Building Accessories (Romania) ASTM International (USA) SAI Global – WaterMark (Australia) Code (Canada) AWWA – American Water EMI – Építésügyi Minőségellenőrző Innovációs (Hungary) SPAN – Suruhanjaya Perkhidmatan Works Association Air Negara (Malaysia) Explosive Environments FESC – Fire Equipment and Safety CSA – CSA Group (Canada) (2014/34/EU) ATEX – Equipment Control Valves Center of Japan SVGW – Schweizerischer Verein des Gas- und Wasserfaches GOST R – Gosstandart (Russia) and protective systems for Hydraulic potentially explosive atmospheres FDNY – Fire Department, (Switzerland) IBC – International Building City of New York (USA) (Europe) UL – Underwriter’s Laboratories, Code (USA) FM – FM Approvals (USA) LLC – NSF 61/372 (USA) ICC – International Code Seismic HDB – Housing Development WRAS – Water Regulations Code (USA) Automatic Board (Singapore) Advisory Scheme (UK) OSHPD – Office of Statewide Health Sprinklers IMC – International Mechanical Planning and Development (USA) KFI – Korea Fire Institute ZUOVA – Zdravotní ústav se sídlem Code (USA) PSB – TÜV SÜD PSB (Singapore) v Ostravě (Czech Republic) IPC – International Plumbing KFSD – Kuwait Fire Service Directorate Code (USA) Maritime Tools and Machinery Safety IRC – International Residential Victaulic LPCB – Loss Prevention Vortex Certification Board (UK) ABS – American Bureau of Shipping Code (USA) (2006/42/EC) MD – Machinery Directive (Europe) SBSC – Svensk Brand- & BV – Bureau Veritas (France) ISO – International Organization ™ Säkerhetscertifiering AB (Sweden) for Standardization (Global) (2014/35/EU) LVD – Low Voltage CCG – Canadian Coast Directive (Europe) TFRI – Tianjin Fire Research Institute Guard (Canada) MSS – Manufacturer's Specialty of Ministry of Public Security (China) Standardization Society (USA) (2014/30/EU) EMC – Systems CRS – Croatian Register Electromagnetic Compatibility TSU – Technický Skúšobný Ústav of Shipping (Croatia) NACE – National Association Directive (Europe) Pieštany, š.p. (Slovakia) of Corrosion Engineers (USA) CCS – China Classification NFPA – National Fire Protection TZUS – Technický a Zkuševní Ústav Society (China) Preparation Pipe Stavební Praha, s.p. (Czech Republic) Association (USA) DNV GL – Det Norske Veritas- ® © Copyright 2018, Victaulic Tools UAE CD – United Arab Emirates Germanischer Lloyd (Norway) UPC – Uniform Plumbing Code (USA) Company. All rights reserved. Civil Defense KRS – Korean Register WSAA – Water Services No part of this Victaulic catalog UKRFIRESERT – State Certification of Shipping (Korea) Association of Australia Center (Ukraine) may be reproduced, stored in a LR – Lloyd’s Register retrieval system, or transmitted, Design Data UL – Underwriter’s of Shipping (UK) in any form or by any means, Laboratories, LLC (USA) electronic, mechanical, photocopy, RINA – Registro Italiano Navale (Italy) recording or otherwise, without ULC – Underwriter’s the prior written permission Laboratories of Canada USCG – US Coast Guard (USA) of Victaulic Company. Index G-105 REV I victaulic.com G-105 REV I Since 1919, Victaulic’s pipe joining and flow control solutions TABLE OF CONTENTS have optimized construction productivity and reduced risk, 1 VicFlex™ Sprinkler Fitting System ensuring projects are completed safely, on time and within 9 Couplings budget. Driven by a spirit of continuous innovation, Victaulic’s 17 Fittings portfolio of 100,000+ products and patented technologies 21 Innovative Groove System (IGS) promote freedom of design, as well as simplified inspection 25 Hole Cut System and maintenance for the life of any system. 27 Valves and Accessories 35 Devices and Accessories Look inside many of the world’s most recognizable landmarks 47 Hydraulic Control Valves and industrial facilities, and you will find Victaulic solutions 53 Automatic Sprinklers at work making bold innovations possible. From the tallest 67 Victaulic Vortex™ buildings to the deepest mines, customers trust our products 69 Specialty Systems to increase overall system durability in the most demanding 73 Pipe Preparation Tools construction projects and operating conditions. 85 Design Data 88 Index From concept to commissioning, Victaulic provides innovative piping products and design services that helps engineer confidence into every build. victaulic.com i G-105 REV I CONTINUING EDUCATION Victaulic® offers a wide variety of continuing education courses. From one-hour seminars to full-day events, these courses provide education on key industry concepts and Victaulic solutions. Created for owners, engineers, contractors, the inspection community, and anyone else seeking to expand their knowledge of Victaulic and the industry surrounding the grooved pipe joining and flow control markets. For more information on the Victaulic Continuing Education Courses or to schedule your training, please contact your local sales representative or email us at: [email protected] ii G-105 REV I VIRTUAL DESIGN AND CONSTRUCTION Drawing, BIM coordination and software solutions for the Victaulic Tools for Revit® provides an intuitive set of commercial construction industry. Victaulic.com/resources- tools that are purposely built to improve pipe routing and software offers an extensive library of CAD files and software fabrication functionality in Revit® 2015 through 2018, product content created in each software’s native platform. including Fabrication Parts. It’s specifically designed to meet the needs of engineers, contractors and pipe fabricators — giving you smarter tools to fabricate faster and route more efficiently. victaulicsoftware.com victaulic.com
Recommended publications
  • Wolf-Rayet Stars in the Small Magellanic Cloud II
    A&A 591, A22 (2016) DOI: 10.1051/0004-6361/201527916 Astronomy c ESO 2016 & Astrophysics Wolf-Rayet stars in the Small Magellanic Cloud II. Analysis of the binaries T. Shenar1, R. Hainich1, H. Todt1, A. Sander1, W.-R. Hamann1, A. F. J. Moffat2, J. J. Eldridge3, H. Pablo2, L. M. Oskinova1, and N. D. Richardson4 1 Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. 24/25, 14476 Potsdam, Germany e-mail: [email protected] 2 Département de physique and Centre de Recherche en Astrophysique du Québec (CRAQ), Université de Montréal, CP 6128, Succ. Centre-Ville, Montréal, Québec, H3C 3J7, Canada 3 Department of Physics, University of Auckland, Private Bag, 92019 Auckland, New Zealand 4 Ritter Observatory, Department of Physics and Astronomy, The University of Toledo, Toledo, OH 43606-3390, USA Received 8 December 2015 / Accepted 30 March 2016 ABSTRACT Context. Massive Wolf-Rayet (WR) stars are evolved massive stars (Mi & 20 M ) characterized by strong mass-loss. Hypothetically, they can form either as single stars or as mass donors in close binaries. About 40% of all known WR stars are confirmed binaries, raising the question as to the impact of binarity on the WR population. Studying WR binaries is crucial in this context, and furthermore enable one to reliably derive the elusive masses of their components, making them indispensable for the study of massive stars. Aims. By performing a spectral analysis of all multiple WR systems in the Small Magellanic Cloud (SMC), we obtain the full set of stellar parameters for each individual component.
    [Show full text]
  • The Wolf-Rayet + of Star Binary AB7: a Warmer in the Small Magellanic Cloud+)
    The Wolf-Rayet + Of star binary AB7: A Warmer in the Small Magellanic Cloud+) Manfred W. Pakull1) & Luciana Bianchi2) 1) Observatoire de Besançon, 25044 Besançon Cedex, France 2) Osservatorio Astronomico di Turino, 10025 Pino Torinese, Italy Summary Strong nebular Hell λ4686 recombination radiation (λ4686/Ηβ = 0.2) has recently been detected in the bright HII region N76 in the Small Magellanic Cloud by Testor & Pakull (1989). The rather symmetric intensity distribution suggests a nebular morphology which consists of a thick outer shell comprising the He*"1* and H+ ionization fronts and a central region of warm, highly ionized gas which is surrounded by a hollow inner shell. The source of the high nebular ionization is identified with the peculiar Wolf-Rayet + Of star spectroscopic binary AB7. Optical and UV spectra (cf. Figure) show in addition to hydrogen and helium absorption lines and the NIII λλ4634-41 complex from the Of star, only broad He II and weak NVemission lines due to the Wolf-Rayet companion. The absence of other diagnostic features qualifies the evolved component as a rare, high-excitation WN star (WN2 or WN1). Subtracting from the optical spectrum of AB7 suitably scaled spectra of SMC Ο stars up to the point that the absorption lines disappeared, suggests that the WN 1 component contributes about 30 % to the total optical light. ' 4000 4500 5000 5500 °' üoö ' iioö t7Ö5 üoö" Wavelength (A) WAVELENGTH (AI Optical and IUE spectra of the 06 IIIf+ WN1 binary AB 7 From the nebular λ4686 flux and the optical brightness of the WN1 star a black body Zanstra temperature of about 80 000 Κ and a luminosity of 106 Lo are derived.
    [Show full text]
  • The Wolf-Rayet + of Star Binary AB7: a Warmer in the Small Magellanic Cloud+)
    The Wolf-Rayet + Of star binary AB7: A Warmer in the Small Magellanic Cloud+) Manfred W. Pakull1) & Luciana Bianchi2) 1) Observatoire de Besançon, 25044 Besançon Cedex, France 2) Osservatorio Astronomico di Turino, 10025 Pino Torinese, Italy Summary Strong nebular Hell λ4686 recombination radiation (λ4686/Ηβ = 0.2) has recently been detected in the bright HII region N76 in the Small Magellanic Cloud by Testor & Pakull (1989). The rather symmetric intensity distribution suggests a nebular morphology which consists of a thick outer shell comprising the He*"1* and H+ ionization fronts and a central region of warm, highly ionized gas which is surrounded by a hollow inner shell. The source of the high nebular ionization is identified with the peculiar Wolf-Rayet + Of star spectroscopic binary AB7. Optical and UV spectra (cf. Figure) show in addition to hydrogen and helium absorption lines and the NIII λλ4634-41 complex from the Of star, only broad He II and weak NVemission lines due to the Wolf-Rayet companion. The absence of other diagnostic features qualifies the evolved component as a rare, high-excitation WN star (WN2 or WN1). Subtracting from the optical spectrum of AB7 suitably scaled spectra of SMC Ο stars up to the point that the absorption lines disappeared, suggests that the WN 1 component contributes about 30 % to the total optical light. ' 4000 4500 5000 5500 °' üoö ' iioö t7Ö5 üoö" Wavelength (A) WAVELENGTH (AI Optical and IUE spectra of the 06 IIIf+ WN1 binary AB 7 From the nebular λ4686 flux and the optical brightness of the WN1 star a black body Zanstra temperature of about 80 000 Κ and a luminosity of 106 Lo are derived.
    [Show full text]
  • Characterization of Solar X-Ray Response Data from the REXIS Instrument Andrew T. Cummings
    Characterization of Solar X-ray Response Data from the REXIS Instrument by Andrew T. Cummings Submitted to the Department of Earth, Atmospheric, and Planetary Sciences in partial fulfillment of the requirements for the degree of Bachelor of Science in Earth, Atmospheric, and Planetary Sciences at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY June 2020 ○c Massachusetts Institute of Technology 2020. All rights reserved. Author................................................................ Department of Earth, Atmospheric, and Planetary Sciences May 18, 2020 Certified by. Richard P. Binzel Professor of Planetary Sciences Thesis Supervisor Certified by. Rebecca A. Masterson Principal Research Scientist Thesis Supervisor Accepted by . Richard P. Binzel Undergraduate Officer, Department of Earth, Atmospheric, and Planetary Sciences 2 Characterization of Solar X-ray Response Data from the REXIS Instrument by Andrew T. Cummings Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on May 18, 2020, in partial fulfillment of the requirements for the degree of Bachelor of Science in Earth, Atmospheric, and Planetary Sciences Abstract The REgolith X-ray Imaging Spectrometer (REXIS) is a student-built instrument that was flown on NASA’s Origins, Spectral Interpretation, Resource Identification, Safety, Regolith Explorer (OSIRIS-REx) mission. During the primary science ob- servation phase, the REXIS Solar X-ray Monitor (SXM) experienced a lower than anticipated solar x-ray count rate. Solar x-ray count decreased most prominently in the low energy region of instrument detection, and made calibrating the REXIS main spectrometer difficult. This thesis documents a root cause investigation intothe cause of the low x-ray count anomaly in the SXM. Vulnerable electronic components are identified, and recommendations for hardware improvements are made to better facilitate future low-cost, high-risk instrumentation.
    [Show full text]
  • The Electric Sun Hypothesis
    Basics of astrophysics revisited. II. Mass- luminosity- rotation relation for F, A, B, O and WR class stars Edgars Alksnis [email protected] Small volume statistics show, that luminosity of bright stars is proportional to their angular momentums of rotation when certain relation between stellar mass and stellar rotation speed is reached. Cause should be outside of standard stellar model. Concept allows strengthen hypotheses of 1) fast rotation of Wolf-Rayet stars and 2) low mass central black hole of the Milky Way. Keywords: mass-luminosity relation, stellar rotation, Wolf-Rayet stars, stellar angular momentum, Sagittarius A* mass, Sagittarius A* luminosity. In previous work (Alksnis, 2017) we have shown, that in slow rotating stars stellar luminosity is proportional to spin angular momentum of the star. This allows us to see, that there in fact are no stars outside of “main sequence” within stellar classes G, K and M. METHOD We have analyzed possible connection between stellar luminosity and stellar angular momentum in samples of most known F, A, B, O and WR class stars (tables 1-5). Stellar equatorial rotation speed (vsini) was used as main parameter of stellar rotation when possible. Several diverse data for one star were averaged. Zero stellar rotation speed was considered as an error and corresponding star has been not included in sample. RESULTS 2 F class star Relative Relative Luminosity, Relative M*R *eq mass, M radius, L rotation, L R eq HATP-6 1.29 1.46 3.55 2.950 2.28 α UMi B 1.39 1.38 3.90 38.573 26.18 Alpha Fornacis 1.33
    [Show full text]
  • The Messenger
    Czech Republic joins ESO The Messenger Progress on ALMA CRIRES Science Verification Gender balance among ESO staff No. 128 – JuneNo. 2007 The Organisation The Czech Republic Joins ESO Catherine Cesarsky The XXVIth IAU General Assembly, held This Agreement was formally confirmed (ESO Director General) in Prague in 2006, clearly provided a by the ESO Council at its meeting on boost for the Czech efforts to join ESO, 6 December and a few days thereafter by not the least in securing the necessary the Czech government, enabling a sign- I am delighted to welcome the Czech public and political support. Thus our ing ceremony in Prague on 22 December Republic as our 13th member state. From Czech colleagues used the opportunity (see photograph below). This was impor- its size, the Czech Republic may not be- to publish a fine and very interesting pop- tant because the Agreement foresaw long to the ‘big’ member states, but the ular book about Czech astronomy and accession by 1 January 2007. With the accession nonetheless marks an impor- ESO, which, together with the General signatures in place, the agreement could tant point in ESO’s history and, I believe, Assembly, created considerable media be submitted to the Czech Parliament in the history of Czech astronomy as well. interest. for ratification within an agreed ‘grace pe- The Czech Republic is the first of the riod’. This formal procedure was con- Central and East European countries to On 20 September 2006, at a meeting at cluded on 30 April 2007, when I was noti- join ESO. The membership underlines ESO Headquarters, the negotiating teams fied of the deposition of the instrument of ESO’s continuing evolution as the prime from ESO and the Czech Republic arrived ratification at the French Ministry of European organisation for astronomy, at an agreement in principle, which was Foreign Affairs.
    [Show full text]
  • The Shortest-Period Wolf-Rayet Binary in the Small Magellanic Cloud: Part of a High-Order Multiple System Spectral and Orbital Analysis of SMC AB 6
    Astronomy & Astrophysics manuscript no. paper c ESO 2018 May 4, 2018 The Shortest-period Wolf-Rayet binary in the Small Magellanic Cloud: Part of a high-order multiple system Spectral and orbital analysis of SMC AB 6 T. Shenar1, R. Hainich1, H. Todt1, A. F. J. Moffat2, A. Sander1, L. M. Oskinova1, V. Ramachandran1, M. Munoz3, H. Pablo5, H. Sana4, and W.-R. Hamann1 1Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam, Germany e-mail: [email protected] 2Département de physique and Centre de Recherche en Astrophysique du Québec (CRAQ), Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, Québec, H3C 3J7, Canada 3Queen’s University 99 University Ave, Kingston, Ontario, Canada 4Institute of Astrophysics, KU Leuven, Celestijnenlaan 200 D, 3001, Leuven, Belgium 5American Association of Variable Star Observers, 49 Bay State Road, Cambridge, MA 02138, USA Received ? / Accepted ? ABSTRACT Context. SMC AB 6 is the shortest-period (P=6:5 d) Wolf-Rayet (WR) binary in the Small Magellanic Cloud. This binary is therefore a key system in the study of binary interaction and formation of WR stars at low metallicity. The WR component in AB 6 was previously found to be very luminous (log L=6:3 [L ]) compared to its reported orbital mass ( 8 M ), placing it significantly above the Eddington limit. ≈ Aims. Through spectroscopy and orbital analysis of newly acquired optical data taken with the Ultraviolet and Visual Echelle Spectrograph (UVES), we aim to understand the peculiar results reported for this system and explore its evolutionary history.
    [Show full text]
  • Arxiv:1902.03928V1 [Astro-Ph.CO] 11 Feb 2019 Keywords: Fine-Tuning, Multiverse, Fundamental Constants, Cosmology, Stellar Evolution, Nucleosynthesis, Habitability
    The Degree of Fine-Tuning in our Universe – and Others Fred C. Adams1;2 1Physics Department, University of Michigan, Ann Arbor, MI 48109, USA 2Astronomy Department, University of Michigan, Ann Arbor, MI 48109, USA Abstract Both the fundamental constants that describe the laws of physics and the cosmolog- ical parameters that determine the properties of our universe must fall within a range of values in order for the cosmos to develop astrophysical structures and ultimately support life. This paper reviews the current constraints on these quantities. The dis- cussion starts with an assessment of the parameters that are allowed to vary. The stan- dard model of particle physics contains both coupling constants (α, αs; αw) and particle masses (mu; md; me), and the allowed ranges of these parameters are discussed first. We then consider cosmological parameters, including the total energy density of the uni- verse (Ω), the contribution from vacuum energy (ρΛ), the baryon-to-photon ratio (η), the dark matter contribution (δ), and the amplitude of primordial density fluctuations (Q). These quantities are constrained by the requirements that the universe lives for a sufficiently long time, emerges from the epoch of Big Bang Nucleosynthesis with an acceptable chemical composition, and can successfully produce large scale structures such as galaxies. On smaller scales, stars and planets must be able to form and func- tion. The stars must be sufficiently long-lived, have high enough surface temperatures, and have smaller masses than their host galaxies. The planets must be massive enough to hold onto an atmosphere, yet small enough to remain non-degenerate, and contain enough particles to support a biosphere of sufficient complexity.
    [Show full text]
  • Comprehensive Analyses of Massive Binaries and Implications on Stellar Evolution
    Institut für Physik und Astronomie Astrophysik I Comprehensive analyses of massive binaries and implications on stellar evolution Kumulative Dissertation zur Erlangung des akademischen Grades “doctor rerum naturalium” (Dr. rer. nat.) in der Wissenschaftsdisziplin Astrophysik eingereicht an der Mathematisch-Naturwissenschaftlichen Fakultät der Universität Potsdam von Tomer Shenar Potsdam, den 02. September 2016 Published online at the Institutional Repository of the University of Potsdam: URN urn:nbn:de:kobv:517-opus4-104857 http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-104857 Abstract (English / Deutsch) Via their powerful radiation, stellar winds, and supernova explosions, massive stars (Mini & 8 M ) bear a tremendous impact on galactic evolution. It became clear in recent decades that the majority of massive stars reside in binary systems. This thesis sets as a goal to quantify the impact of binarity (i.e., the presence of a companion star) on massive stars. For this purpose, massive binary systems in the Local Group, including OB-type binaries, high mass X-ray binaries (HMXBs), and Wolf-Rayet (WR) binaries, were investigated by means of spectral, orbital, and evolutionary analyses. The spectral analyses were performed with the non-local thermodynamic equillibrium (non-LTE) Pots- dam Wolf-Rayet (PoWR) model atmosphere code. Thanks to critical updates in the calculation of the hydrostatic layers, the code became a state-of-the-art tool applicable for all types of hot massive stars (Chapter 2). The eclipsing OB-type triple system δ Ori served as an intriguing test-case for the new version of the PoWR code, and provided key insights regarding the formation of X-rays in massive stars (Chapter 3).
    [Show full text]
  • The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables
    The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turn-offs. I. Results from 19 OB Associations in the Magellanic Clouds PHILIP MASSEY1 Kitt Peak National Observatory, National Optical Astronomy Observatories2 P.O. Box 26732, Tucson, AZ 85726-6732 ELIZABETH WATERHOUSE3 and KATHLEEN DEGIOIA-EASTWOOD Department of Physics and Astronomy, Northern Arizona University, P.O. Box 6010, Flagstaff, AZ 86011-6010. Received ; accepted arXiv:astro-ph/0002233v1 10 Feb 2000 1Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. 2Operated by AURA under cooperative agreement with the National Science Foundation. 3Participant in Research Experiences for Undergraduates program, Northern Arizona University, Summer 1998. Present address: Harvard University, 436 Eliot House Mail Center, 101 Dunster St., Cambridge, MA 02138. –2– ABSTRACT We combine new CCD UBV photometry and spectroscopy with that from the literature to investigate 19 Magellanic Cloud OB associations that contain Wolf-Rayet (WR) and other types of evolved massive stars. Our spectroscopy reveals a wealth of newly identified interesting objects, including early O-type supergiants, a high mass double-lined binary in the SMC, and, in the LMC, a newly confirmed LBV (R 85), a newly discovered WR star (Sk−69◦194), and a newly found luminous B[e] star (LH85-10). We use these data to provide precise reddening determinations and construct physical H-R diagrams for the associations. We find that about half of the associations may be highly coeval, with the massive stars having formed over a short period (∆τ < 1 Myr).
    [Show full text]
  • Elenco Device Android.Xlsx
    Manufacturer,Model Name,Model Code,RAM (TotalMem),Form Factor,System on Chip,Screen Sizes,Screen Densities,ABIs,Android SDK Versions,OpenGL ES Versions 10.or,10or_G2,G2,3742-5747MB,Phone,Qualcomm SDM636,1080x2246,480,arm64-v8a 10.or,E,E,1857-2846MB,Phone,Qualcomm MSM8937,1080x1920,480,arm64-v8a 10.or,G,G,2851-3582MB,Phone,Qualcomm MSM8953,1080x1920,480,arm64-v8a 10.or,D,10or_D,2868-2874MB,Phone,Qualcomm MSM8917,720x1280,320,arm64-v8a 7mobile,SWEGUE,SWEGUE,1836MB,Phone,Mediatek MT6737T,1080x1920,480,arm64-v8a 7mobile,Kamba 2,7mobile_Kamba_2,2884MB,Phone,Mediatek MT6739CH,720x1440,320,arm64-v8a A1,A1 Alpha 20+,P671F60,3726MB,Phone,Mediatek MT6771T,1080x2340,480,arm64-v8a Accent,FAST10,FAST10,1819MB,Tablet,Spreadtrum SC9863A,1280x800,213,arm64-v8a ACE France,BUZZ 2,BUZZ_2,850MB,Phone,Spreadtrum SC9863A,720x1560,320,armeabi-v7a ACE France,BUZZ 2,BUZZ_2_Plus,1819MB,Phone,Spreadtrum SC9863A,720x1560,320,arm64-v8a ACE France,URBAN 2,URBAN_2,2824MB,Phone,Spreadtrum SC9863A,720x1560,320,arm64-v8a ACE France,AS0518,AS0518,1822MB,Phone,Mediatek MT6762,720x1440,320,arm64-v8a ACE France,URBAN 1,URBAN_1,1839MB,Phone,Mediatek MT6739WA,720x1440,320,arm64-v8a ACE France,AS0618,AS0618,2826MB,Phone,Mediatek MT6752,720x1500,320,arm64-v8a Acer,Iconia Tab 10,acer_asgard,1970MB,Tablet,Mediatek MT8176A,800x1280,160,arm64-v8a Acer,Iconia Tab 10,acer_asgardfhd,1954MB,Tablet,Mediatek MT8167B,1920x1200,240,arm64-v8a Acer,Iconia Tab 10,acer_Titan,3959MB,Tablet,Mediatek MT8176A,1200x1920,240,arm64-v8a Acer,Liquid Z530S,acer_t05,2935MB,Phone,Mediatek MT6753,720x1280,320,arm64-v8a
    [Show full text]
  • An X-Ray Investigation of the NGC346 Field in the SMC (1): the LBV
    An X-ray investigation of the NGC 346 field in the SMC (1) : the LBV HD 5980 and the NGC 346 cluster Y. Naz´e1,8, J.M. Hartwell2, I.R. Stevens2, M. F. Corcoran3, Y.-H. Chu4, G. Koenigsberger5, A.F.J. Moffat6, V.S. Niemela7 ABSTRACT We present results from a Chandra observation of the NGC 346 cluster. This cluster contains numerous massive stars and is responsible for the ionization of N66, the most luminous H ii region and the largest star formation region in the SMC. In this first paper, we will focus on the characteristics of the main objects of the field. The NGC 346 cluster itself shows only relatively unabs 34 −1 faint X-ray emission (with LX ∼ 1.5 × 10 erg s ), tightly correlated with the core of the cluster. In the field also lies HD 5980, a LBV star in a binary (or possibly a triple system) that is detected for the first time at X-ray energies. The star is X-ray bright, with an unabsorbed unabs 34 −1 luminosity of LX ∼ 1.7 × 10 erg s , but needs to be monitored further to investigate its X-ray variability over a complete 19 d orbital cycle. The high X-ray luminosity may be associated either with colliding winds in the binary system or with the 1994 eruption. HD 5980 is surrounded by a region of diffuse X-ray emission, which is a supernova remnant. While it may be only a chance alignment with HD 5980, such a spatial coincidence may indicate that the remnant is indeed related to this peculiar massive star.
    [Show full text]